\relax 
\bibstyle{mn2e}
\citation{springel05nb,boylan08,klypin11,angulo12}
\citation{2014arXiv1409.8617S,2013MNRAS.431.1366S,2014arXiv1412.2748S,2014MNRAS.439.2485C,2014MNRAS.442.2641V,2014MNRAS.444.1518V}
\citation{white78,fall80}
\citation{katz96,springel03,keres05,crain09,schaye10,oppenheimer10}
\citation{kauffmann99,springel01,hatton03,springelsam05,kang05,croton06,bower06,guo11}
\citation{vale04,conroy06,shankar06,vale06,moster10,guo10,behroozi10,moster13}
\citation{strateva01,blanton03,kauffmann03,madgwick03}
\@writefile{toc}{\contentsline {section}{\numberline {1}INTRODUCTION}{1}}
\newlabel{sec:intro}{{1}{1}}
\citation{2006MNRAS.365...11C,2006MNRAS.370..645B,2006MNRAS.368....2D,2006MNRAS.370.1651C,2008ApJS..175..390H}
\citation{1972ApJ...176....1G,1998ApJ...495..139M,2000ApJ...540..113B}
\citation{moster10}
\citation{yang03}
\citation{moster10}
\@writefile{toc}{\contentsline {section}{\numberline {2}Numerical Simulations and Observational Data}{2}}
\newlabel{sec:data}{{2}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.1}Numerical Simulations}{2}}
\newlabel{sub:sims}{{2.1}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.2}Observational Data}{2}}
\newlabel{sub:data}{{2.2}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Modeling}{2}}
\newlabel{sec:modeling}{{3}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Stellar-to-Halo Mass Relation}{2}}
\newlabel{sub:shm}{{3.1}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.2}Active Fraction}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces The functional form used for the stellar-to-halo mass relation. \textit  {Above:} Stellar mass vs. halo mass. $1+\beta $ is the low-mass slope, $1-\gamma $ is the high-mass slope, $M_1$ is the characteristic halo mass where the slope changes, and $N\cdot M_1$ is the stellar mass at $M_1$. \textit  {Below:} The same relationship, expressed as the ratio of stellar to halo mass (i.e. stellar mass fraction) vs. halo mass. The low- and high-mass slopes are $\beta $ and $-\gamma $, respectively, $M_1$ is the characteristic halo mass, and $N$ is the stellar mass fraction at that halo mass. The horizontal dotted line represents the value of the universal baryon fraction, the maximum physically allowable value of this ratio (this value would represent a situation where all baryons are in stars and there is no gas or dust.)}}{3}}
\newlabel{shm_motiv}{{1}{3}}
\newlabel{eq:expform}{{2}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces  {\bf  [ARZ: The first line of a caption should be some sort of title or introduction to the figure and is not required to be a complete sentence. For example, one might choose ``Active galaxy fractions in SDSS groups" for the first line of this caption. You should specify how the errors are computed. You also need to show the best fit parameter of the model. I would actually write the functional form directly in the upper right of the figure as a legend would appear and not in that region of the plot the best-fit parameter value.]} In dark blue, the fraction of galaxies per halo mass bin that are active, with the light blue representing a 95\% confidence interval due to cosmic variance. The halo masses come from an abundance matching, with the corresponding galaxies from an SDSS catalog. The green line shows a fit with our functional form, demonstrating that our functional form can approximate the observed trend \leavevmode {\color  {red}}}}{3}}
\newlabel{pb_motiv}{{2}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.3}Subhalos}{3}}
\newlabel{sub:subhalos}{{3.3}{3}}
\citation{moster10}
\citation{springel05nb}
\citation{millannounce}
\citation{moster10}
\@writefile{toc}{\contentsline {section}{\numberline {4}Results}{4}}
\newlabel{sec:results}{{4}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {4.1}Comparison to Previous Work}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces The ratio of $M_\textrm  {200}$ calculated based on $M_\textrm  {vir}$ calculated in ROCKSTAR to $M_\textrm  {200}$ calculated in ROCKSTAR for halos in Bolshoi. The thick black line represents the median ratio at a particular ROCKSTAR $M_\textrm  {200}$, and the dark and light blue regions represent 68\% and 95\% confidence intervals, respectively, at a particular value on the x axis. The horizontal blue dotted line at 1.0 is for reference and represents an exact match between the two values. The conversion prescription works well for halos larger than about $2 \times 10^9 M_\odot $.}}{5}}
\newlabel{massrat}{{3}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces The inferred stellar-to-halo mass relationship. The thick green line is the best fit; the thin blue lines represent alternate models that are within a 1$\sigma $ deviation from the best fit, chosen at random. The dotted lines represent models that are at least a 1$\sigma $ deviation from the best fit but no more than a 2$\sigma $ deviation. }}{5}}
\newlabel{SHM}{{5}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces The inferred blue fraction as a function of halo mass, plotted in the same way as Fig. 5\hbox {}. \leavevmode {\color  {red}annotation?}}}{5}}
\newlabel{Pb}{{6}{5}}
\@writefile{toc}{\contentsline {section}{\numberline {5}Discussion}{5}}
\newlabel{sec:discussion}{{5}{5}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces The maximum likelihood values for the six model parameters and 95\% confidence interval, according to the posterior of our MCMC. \leavevmode {\color  {red}}}}{6}}
\newlabel{maxlik}{{1}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Posterior probability distribution for the six parameters in our model. The blue horizontal and vertical lines with a point at the intersection represent one of the samples with the highest likelihood, $\chi ^2 = 46.4$. \leavevmode {\color  {red}}}}{6}}
\newlabel{triangle}{{4}{6}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces Comparison of median parameter values with 68\% confidence intervals for Bolshoi vs. Millennium. The third row shows the best fit and 1$\sigma $ confidence intervals derived by Moster et al. 2010. \leavevmode {\color  {red}Need to add my own millennium/sdss results}. \leavevmode {\color  {red}}}}{6}}
\newlabel{millennium}{{2}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Above: The red stellar mass function predicted by the maximum likelihood model. The points with error bars represent the PRIMUS data used to constrain our model. The thick black line represents the best fit model - the thin red lines represent alternate models, chosen at random, that are less than a 1$\sigma $ deviation from the maximum likelihood. The dashed lines represent a deviation from the maximum likelihood of at least 1$\sigma $ but no more than 2$\sigma $. Below: The blue stellar mass function predictions, plotted in the same way. \leavevmode {\color  {red}}}}{7}}
\newlabel{SMF}{{7}{7}}
\bibstyle{plainnat}
\bibdata{N-body,AM,galaxyform,hydro,sam,baryonMh,galaxybi,quenching}
\bibcite{angulo12}{{1}{2012}{{{Angulo} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Angulo}, {Springel}, {White}, {Jenkins}, {Baugh}, \& {Frenk}}}}
\bibcite{2000ApJ...540..113B}{{2}{2000}{{{Balogh}, {Navarro} \& {Morris}}}{{{Balogh}, {Navarro}, \& {Morris}}}}
\bibcite{behroozi10}{{3}{2010}{{{Behroozi}, {Conroy} \& {Wechsler}}}{{{Behroozi}, {Conroy}, \& {Wechsler}}}}
\bibcite{blanton03}{{4}{2003}{{{Blanton} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Blanton}, {Hogg}, {Bahcall}, {Baldry}, {Brinkmann}, {Csabai}, {Eisenstein}, {Fukugita}, {Gunn}, {Ivezi{\'c}}, {Lamb}, {Lupton}, {Loveday}, {Munn}, {Nichol}, {Okamura}, {Schlegel}, {Shimasaku}, {Strauss}, {Vogeley}, \& {Weinberg}}}}
\bibcite{bower06}{{5}{2006{a}}{{{Bower} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Bower}, {Benson}, {Malbon}, {Helly}, {Frenk}, {Baugh}, {Cole}, \& {Lacey}}}}
\bibcite{2006MNRAS.370..645B}{{6}{2006{b}}{{{Bower} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Bower}, {Benson}, {Malbon}, {Helly}, {Frenk}, {Baugh}, {Cole}, \& {Lacey}}}}
\bibcite{boylan08}{{7}{2008}{{{Boylan-Kolchin}, {Ma} \& {Quataert}}}{{{Boylan-Kolchin}, {Ma}, \& {Quataert}}}}
\bibcite{2006MNRAS.370.1651C}{{8}{2006}{{{Cattaneo} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Cattaneo}, {Dekel}, {Devriendt}, {Guiderdoni}, \& {Blaizot}}}}
\bibcite{conroy06}{{9}{2006}{{{Conroy}, {Wechsler} \& {Kravtsov}}}{{{Conroy}, {Wechsler}, \& {Kravtsov}}}}
\bibcite{crain09}{{10}{2009}{{{Crain} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Crain}, {Theuns}, {Dalla Vecchia}, {Eke}, {Frenk}, {Jenkins}, {Kay}, {Peacock}, {Pearce}, {Schaye}, {Springel}, {Thomas}, {White}, \& {Wiersma}}}}
\bibcite{croton06}{{11}{2006{a}}{{{Croton} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Croton}, {Springel}, {White}, {De Lucia}, {Frenk}, {Gao}, {Jenkins}, {Kauffmann}, {Navarro}, \& {Yoshida}}}}
\bibcite{2006MNRAS.365...11C}{{12}{2006{b}}{{{Croton} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Croton}, {Springel}, {White}, {De Lucia}, {Frenk}, {Gao}, {Jenkins}, {Kauffmann}, {Navarro}, \& {Yoshida}}}}
\bibcite{2014MNRAS.439.2485C}{{13}{2014}{{{Cusworth} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Cusworth}, {Kay}, {Battye}, \& {Thomas}}}}
\bibcite{2006MNRAS.368....2D}{{14}{2006}{{{Dekel} \& {Birnboim}}}{{}}}
\bibcite{fall80}{{15}{1980}{{{Fall} \& {Efstathiou}}}{{}}}
\bibcite{1972ApJ...176....1G}{{16}{1972}{{{Gunn} \& {Gott}}}{{}}}
\bibcite{guo11}{{17}{2011}{{{Guo} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Guo}, {White}, {Boylan-Kolchin}, {De Lucia}, {Kauffmann}, {Lemson}, {Li}, {Springel}, \& {Weinmann}}}}
\bibcite{guo10}{{18}{2010}{{{Guo} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Guo}, {White}, {Li}, \& {Boylan-Kolchin}}}}
\bibcite{hatton03}{{19}{2003}{{{Hatton} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Hatton}, {Devriendt}, {Ninin}, {Bouchet}, {Guiderdoni}, \& {Vibert}}}}
\bibcite{2008ApJS..175..390H}{{20}{2008}{{{Hopkins} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Hopkins}, {Cox}, {Kere{\v s}}, \& {Hernquist}}}}
\bibcite{kang05}{{21}{2005}{{{Kang} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Kang}, {Jing}, {Mo}, \& {B{\"o}rner}}}}
\bibcite{katz96}{{22}{1996}{{{Katz}, {Weinberg} \& {Hernquist}}}{{{Katz}, {Weinberg}, \& {Hernquist}}}}
\bibcite{kauffmann99}{{23}{1999}{{{Kauffmann} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Kauffmann}, {Colberg}, {Diaferio}, \& {White}}}}
\bibcite{kauffmann03}{{24}{2003}{{{Kauffmann} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Kauffmann}, {Heckman}, {White}, {Charlot}, {Tremonti}, {Peng}, {Seibert}, {Brinkmann}, {Nichol}, {SubbaRao}, \& {York}}}}
\bibcite{keres05}{{25}{2005}{{{Kere{\v s}} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Kere{\v s}}, {Katz}, {Weinberg}, \& {Dav{\'e}}}}}
\bibcite{klypin11}{{26}{2011}{{{Klypin}, {Trujillo-Gomez} \& {Primack}}}{{{Klypin}, {Trujillo-Gomez}, \& {Primack}}}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces The overall stellar mass function predicted by the maximum likelihood model, plotted in the same way as Fig. 7\hbox {}. The points with error bars are the sums of red and blue data from PRIMUS. These sums were not used in our calculations but are shown here for reference. \leavevmode {\color  {red}color?}}}{8}}
\newlabel{totSMF}{{8}{8}}
\@writefile{toc}{\contentsline {section}{\numberline {6}Acknowledgements}{8}}
\bibcite{millannounce}{{27}{2006}{{{Lemson} \& {Virgo Consortium}}}{{}}}
\bibcite{madgwick03}{{28}{2003}{{{Madgwick} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Madgwick}, {Somerville}, {Lahav}, \& {Ellis}}}}
\bibcite{1998ApJ...495..139M}{{29}{1998}{{{Moore}, {Lake} \& {Katz}}}{{{Moore}, {Lake}, \& {Katz}}}}
\bibcite{moster13}{{30}{2013}{{{Moster}, {Naab} \& {White}}}{{{Moster}, {Naab}, \& {White}}}}
\bibcite{moster10}{{31}{2010}{{{Moster} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Moster}, {Somerville}, {Maulbetsch}, {van den Bosch}, {Macci{\`o}}, {Naab}, \& {Oser}}}}
\bibcite{oppenheimer10}{{32}{2010}{{{Oppenheimer} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Oppenheimer}, {Dav{\'e}}, {Kere{\v s}}, {Fardal}, {Katz}, {Kollmeier}, \& {Weinberg}}}}
\bibcite{2013MNRAS.431.1366S}{{33}{2013}{{{Sawala} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Sawala}, {Frenk}, {Crain}, {Jenkins}, {Schaye}, {Theuns}, \& {Zavala}}}}
\bibcite{2014arXiv1412.2748S}{{34}{2014}{{{Sawala} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Sawala}, {Frenk}, {Fattahi}, {Navarro}, {Bower}, {Crain}, {Dalla Vecchia}, {Furlong}, {Helly}, {Jenkins}, {Oman}, {Schaller}, {Schaye}, {Theuns}, {Trayford}, \& {White}}}}
\bibcite{2014arXiv1409.8617S}{{35}{2014}{{{Schaller} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Schaller}, {Frenk}, {Bower}, {Theuns}, {Jenkins}, {Schaye}, {Crain}, {Furlong}, {Dalla Vecchia}, \& {McCarthy}}}}
\bibcite{schaye10}{{36}{2010}{{{Schaye} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Schaye}, {Dalla Vecchia}, {Booth}, {Wiersma}, {Theuns}, {Haas}, {Bertone}, {Duffy}, {McCarthy}, \& {van de Voort}}}}
\bibcite{shankar06}{{37}{2006}{{{Shankar} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Shankar}, {Lapi}, {Salucci}, {De Zotti}, \& {Danese}}}}
\bibcite{springelsam05}{{38}{2005}{{{Springel}, {Di Matteo} \& {Hernquist}}}{{{Springel}, {Di Matteo}, \& {Hernquist}}}}
\bibcite{springel03}{{39}{2003}{{{Springel} \& {Hernquist}}}{{}}}
\bibcite{springel05nb}{{40}{2005}{{{Springel} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Springel}, {White}, {Jenkins}, {Frenk}, {Yoshida}, {Gao}, {Navarro}, {Thacker}, {Croton}, {Helly}, {Peacock}, {Cole}, {Thomas}, {Couchman}, {Evrard}, {Colberg}, \& {Pearce}}}}
\bibcite{springel01}{{41}{2001}{{{Springel}, {Yoshida} \& {White}}}{{{Springel}, {Yoshida}, \& {White}}}}
\bibcite{strateva01}{{42}{2001}{{{Strateva} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Strateva}, {Ivezi{\'c}}, {Knapp}, {Narayanan}, {Strauss}, {Gunn}, {Lupton}, {Schlegel}, {Bahcall}, {Brinkmann}, {Brunner}, {Budav{\'a}ri}, {Csabai}, {Castander}, {Doi}, {Fukugita}, {Gy{\H o}ry}, {Hamabe}, {Hennessy}, {Ichikawa}, {Kunszt}, {Lamb}, {McKay}, {Okamura}, {Racusin}, {Sekiguchi}, {Schneider}, {Shimasaku}, \& {York}}}}
\bibcite{vale04}{{43}{2004}{{{Vale} \& {Ostriker}}}{{}}}
\bibcite{vale06}{{44}{2006}{{{Vale} \& {Ostriker}}}{{}}}
\bibcite{2014MNRAS.442.2641V}{{45}{2014}{{{Velliscig} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Velliscig}, {van Daalen}, {Schaye}, {McCarthy}, {Cacciato}, {Le Brun}, \& {Dalla Vecchia}}}}
\bibcite{2014MNRAS.444.1518V}{{46}{2014}{{{Vogelsberger} {et~al}\unhbox \voidb@x \hbox {.}}}{{{Vogelsberger}, {Genel}, {Springel}, {Torrey}, {Sijacki}, {Xu}, {Snyder}, {Nelson}, \& {Hernquist}}}}
\bibcite{white78}{{47}{1978}{{{White} \& {Rees}}}{{}}}
\bibcite{yang03}{{48}{2003}{{{Yang}, {Mo} \& {van den Bosch}}}{{{Yang}, {Mo}, \& {van den Bosch}}}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces This correlation function plot is a placeholder, and requires a number of additions and aesthetic improvements. The dotted line refers to APH's age-matching results.}}{9}}
\newlabel{correlation}{{9}{9}}
